Formation of Low Mass Stars, Disks, and Outflows

Details Formation of Low Mass Stars, Disks, and Outflows Formation of Low Mass Stars, Disks, and Outflows

Aug 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007jena.confr..15m&link_type=abstract

"JENAM-2007, "Our non-stable Universe", held 20-25 August 2007 in Yerevan, Armenia. Abstract book, p. 15-15"

Computer Science

Scientific paper

We are studied the super fine structure of the Orion-KL active region of H2O maser emission V=7.65 km/s in polarized emission with angular resolution 0.15 mas or 0.07 AU, epoch 1998-1999. The star formation is accompanied by a structure that consists of bright compact source - ejector, high-collimated bipolar outflow and torus-disk, divided into protoplanetary rings. Brightness temperature of the ejector Tb = 10^17 K, degree of linear ploarization is m~50%. The ring rotation corresponds to hard disk. Rotation period is equal 170 yr. Precession of axies (T~10yr) is determined helix structure of the outflow. Variation of the polarized plane in the profile is equal dX/dV = - 23 deg/km/s, that is much higher than Faraday's rotation in the HII region in front of the molecular cloud. The “rotation” is effect of different polarized orientation of bipolar ejector.

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